Ices in Starless and Starforming Cores

Icy grain mantles are commonly observed through infrared spectroscopy toward dense clouds, cloud cores, protostellar envelopes and protoplanetary disks. Up to 80% of the available oxygen, carbon and nitrogen are found in such ices; the most common ice constituents – H2O, CO2 and CO – are second in a...

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Bibliographic Details
Published in:Proceedings of the International Astronomical Union 2011-06, Vol.7 (S280), p.65-78
Main Authors: Öberg, Karin I., Boogert, A. C. Adwin, Pontoppidan, Klaus M., van den Broek, Saskia, van Dishoeck, Ewine F., Bottinelli, Sandrine, Blake, Geoffrey A., Evans, Neal J.
Format: Article
Language:English
Subjects:
Astrobiology
Astrophysics
Chemistry
Contributed Papers
Ice
Molecules
Star & galaxy formation
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Summary:Icy grain mantles are commonly observed through infrared spectroscopy toward dense clouds, cloud cores, protostellar envelopes and protoplanetary disks. Up to 80% of the available oxygen, carbon and nitrogen are found in such ices; the most common ice constituents – H2O, CO2 and CO – are second in abundance only to H2 in many star forming regions. In addition to being a molecular reservoir, ice chemistry is responsible for much of the chemical evolution from H2O to complex, prebiotic molecules. Combining the exisiting ISO, Spitzer, VLT and Keck ice data results in a large sample of ice sources (~80) that span all stages of star formation and a large range of protostellar luminosities (
ISSN:1743-9213
1743-9221
DOI:10.1017/S1743921311024872